Date and Time of the Query: 2018-12-11 T05:51:20 PST
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Notes for object NGC 4526

14 note(s) found in NED.

1. 2006MNRAS.369..497K
Re:NGC 4526
This S0 object has a prominent dust disc which is not only visible in the
reconstructed SAURON image but also clearly seen in the Mg b and H{beta} maps.
The strong H{beta} line strengths in the region of the dust lane indicate the
presence of dust enshrouded young stars.

2. 2006MNRAS.366.1151S
Re:NGC 4526
Another prototypical example of an early-type galaxy with a perfect dust disc,
very regular gas kinematics, a circumnuclear region where H{beta} emission is
particularly strong, and an independently derived H{beta} kinematics indicating
faster rotation and smaller velocity dispersions than the [O III] kinematics. As
in NGC 3032 and 4459, molecular gas was detected by Sage & Wrobel (1989).

3. 2006ApJS..164..334F
Re:VCC 1535
VCC 1535 (NGC 4526).This galaxy hosts a large dust disk, very reminiscent of the
one seen, at lower inclination, in VCC 1154. The disk extends 15.6" on
either side of the galaxy's center and is aligned with the major axis of the
galaxy (in the east-southeast direction). The plane of the disk makes an angle
of approximately 15^deg^ to the line of sight,the northern side being the
There are several blue knots within the disk, probably indicative of star
formation. Because the underlying stellar population within the disk is likely
different from that characterizing the main body of the galaxy, the dust
correction for this galaxy fails, and the isophotes can only be recovered
outside a semimajor axis of 7". At a radius of approximately 10"
the isophotes become visibly boxy; the boxiness is rather extreme at a radius of
20". Beyond, the isophotes assume a diamond shape appearance (as a
consequence the A4 coefficient becomes nonzero), and finally become disky at a
radius of approximately 70".

4. 2004MNRAS.352..721E
Re:NGC 4526
NGC 4526: This S0 object has a prominent dust disc which is not only
visible in the reconstructed SAURON image, but also influences the
observed kinematics. The dumbbell shape in the dispersion map is due to
a fast rotating stellar component, well visible in the velocity map. The
data of Pellegrini, Held & Ciotti (1997) also shows the drop in velocity
between 10 and 20 arcsec, which corresponds to this component. h_3_
reverses sign at about 20 arcsec along the major axis.

5. 2002AJ....124..675C
Re:UGC 07718
Unusually high FIR/radio flux ratio.

6. 1999AJ....118.2331V
Re:NGC 4526
A set of short- and long-exposure F555W and F814W images is
available. SN Ia 1994D is clearly seen on the HST images; it occurred
along the edge of the central dusty disk of this host galaxy, just
beyond or north of the prominent dust lanes (Fig. 23). Although the SN
is saturated in the long-exposure images, only the central pixels of the
SN profile are saturated in the shorter exposures.
We have measured the magnitudes of the SN in the two HST filters by
using the wings of the stellar profile and interpolating the flux lost
in the saturated portion of the profile. We used the unsaturated
magnitudes of the field star (which is "star C" in Richmond et al.
1995), also seen on the image, as a reference. We find
m_F555W_ = 14.48 +/- 0.08 and m_F814W_ = 14.19 +/- 0.08 mag for SN 1994D
on 1994 May 9 UT. These values agree well with V = 14.40 and I = 14.19
mag for 1994 May 8 UT by Richmond et al. (Our measurements for the field
star magnitudes, m_F555W_ = 16.35 and m_F814W_ = 15.51 mag, also agree
well with Richmond et al.'s magnitudes for this star.)
The SN environment is dominated by diffuse starlight in the host
galaxy. We averaged the measurements of the magnitude and color of the
SN environment on the deeper images through two 0.5" -radius apertures,
placed on either side of (and outside) the wings of the saturated SN
PSF. We find that m_F555W_ = 19.40 and F555W - F814W = 1.52 mag in the
environment, which is quite red. Undoubtedly, dust must be contributing
to the colors of this environment, but taken at face value, the color
implies the presence of K-type stars, presumably giants, in the SN
environment in this early-type host galaxy.

7. 1994CAG1..B...0000S
Re:NGC 4526
VCC 1535
Hubble Atlas, p. 5
Feb 24/25, 1979
103aO + Wr2c
45 min
The print of NGC 4526 in the Hubble Atlas, made from a Mount
Wilson 60-inch plate, shows the internal, S0_3_-characteristic ring
that is buried very deep in the main body of the image. The 60-inch
plate, printed at great enlargement in the Hubble Atlas, clearly shows
that the circular internal structure is obscuration rather than a
bright rim, in contrast to the cases of NGC 148 and NGC 4124, also on
this panel.

8. 1994A&AS..106..199C
Re:NGC 4526
NGC 4526. It hosts an inner dust lane parallel to the major axis,
extending out to ~20" from the nucleus.

9. 1994A&AS..105..481M
Re:NGC 4526
NGC 4526: This has been classified from literature data by Liller,
1960, Michard, 1985 and also the photo in WCAG. This edge-on system shows
a boxy bulge, somewhat asymmetric, with indication of spiral structure in
a limited range. Wray interprets these features as indicative of a barred
spiral with the bar nearly end-on. The envelope classification is very
uncertain, between thD and spH, mainly because the axis-ratio
measurements of the above quoted authors are not in good agreement for
the outermost range.

10. 1976RC2...C...0000d
Re:NGC 4526
Ap. J., 146, 28, 1966.
Photometry (5 Color):
A.J., 73, 313, 1968.
IAU Circ. No. 2139, 1969.

11. 1973UGC...C...0000N
Re:UGC 07718
SAB(s)0/a: (de Vaucouleurs)
SN 1969e

12. 1964RC1...C...0000d
Re:NGC 4526
Small, bright diffuse nucleus in a bright diffuse inner lens: 0.55 arcmin x
0.4 arcmin with a dark crescent simulating (r). Bright foreshortened bar,
in a lens: 2.9 arcmin x 0.7 arcmin. Faint envelope.
Ap. J., 120, 444, 1954.
B.A.N., 16, 1, 1961.
M.N.R.A.S., 94, 806, 1934.
Ap. J., 120, 439, 1954.
Ap. J., 132, 305, 1960.
B.A.N., 16, 1, 1961.
Radio Emission:
Observatory, 80, 216, 1960.
M.N.R.A.S., 123, 279, 1961.

13. 1961Hubbl.B...0000S
Re:NGC 4526
Feb. 12/13, 1939
Imp. Ecl.
60 min
Enlarged 10.0X
NGC 4526 is a good example of an S03 seen at a large
projection angle. The internal ring is blocked on the far side
by the spherical nucleus projecting in front of the ring.
A very large outer envelope, characteristic of S01, can
be traced on the original negative for a distance of 230
sec of arc, which corresponds to 85 mm on this illustration.

14. 1918PLicO..13....9C
Re:NGC 4526
5' x 1' in p.a. 112^deg^; very bright central portion with a somewhat elongated
nucleus, near which is a clear-cut, curved absorption lane. No whorls
distinguishable. See Abs. Eff. 17 s.n.

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